Inner Polar Disks and Rings: How Do They Form?

Details Inner Polar Disks and Rings: How Do They Form? Inner Polar Disks and Rings: How Do They Form?

Jun 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aipc.1240..251m&link_type=abstract

HUNTING FOR THE DARK: THE HIDDEN SIDE OF GALAXY FORMATION. Edited by Victor P. Debattista and Cristina C. Popescu AIP Conferen

Physics

4

Galaxies, Stellar Structure, Accretion, Merging, Origin, Formation, Evolution, Age, And Star Formation, Stellar Content And Populations, Radii, Morphology And Overall Structure, Infall, Accretion, And Accretion Disks, Galaxy Mergers, Collisions, And Tidal Interactions

Scientific paper

Inner polar disks and rings with sizes from 100 pc to 1 kpc have been recently found in some nearby galaxies. Most of these structures were detected only from their kinematical tracers being hard to be noticed against the high-brightness bulges. Starting from 1990s the number of kinematically confirmed inner polar structures (IPS) increased, but their origin and evolution is not understood yet. We have collected a new list of galaxies with IPS; their sample properties are discussed here.

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